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A Hot Terrestrial Planet Orbiting the Bright M Dwarf L 168-9 Unveiled by TESS ?,??,??? N

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A Hot Terrestrial Planet Orbiting the Bright M Dwarf L 168-9 Unveiled by TESS ?,??,??? N A&A 636, A58 (2020) Astronomy https://doi.org/10.1051/0004-6361/201937179 & © ESO 2020 Astrophysics A hot terrestrial planet orbiting the bright M dwarf L 168-9 unveiled by TESS ?,??,??? N. Astudillo-Defru1, R. Cloutier2,3, S. X. Wang4, J. Teske4,????, R. Brahm5,6,7, C. Hellier8, G. Ricker9, R. Vanderspek9, D. Latham2, S. Seager10, J. N. Winn11, J. M. Jenkins12, K. A. Collins2, K. G. Stassun13, C. Ziegler14, J. M. Almenara15, D. R. Anderson8,16, E. Artigau17, X. Bonfils15, F. Bouchy18, C. Briceño19, R. P. Butler20, D. Charbonneau2, D. M. Conti21, J. Crane4, I. J. M. Crossfield22,23, M. Davies12, X. Delfosse15, R. F. Díaz24,25, R. Doyon17, D. Dragomir26, J. D. Eastman2, N. Espinoza27, Z. Essack10, F. Feng20, P. Figueira28,41, T. Forveille15, T. Gan30, A. Glidden9, N. Guerrero9, R. Hart31, Th. Henning32, E. P. Horch33, G. Isopi34, J. S. Jenkins35, A. Jordán36,7, J. F. Kielkopf37, N. Law38, C. Lovis18, F. Mallia34, A. W. Mann38, J. R. de Medeiros39, C. Melo28, R. E. Mennickent29, L. Mignon15, F. Murgas15, D. A. Nusdeo40, F. Pepe18, H. M. Relles2, M. Rose12, N. C. Santos41,42, D. Ségransan18, S. Shectman4, A. Shporer9, J. C. Smith43,12, P. Torres5, S. Udry18, J. Villasenor44, J .G. Winters2, and G. Zhou2 (Affiliations can be found after the references) Received 22 November 2019 / Accepted 27 January 2020 ABSTRACT We report the detection of a transiting super-Earth-sized planet (R = 1.39 0.09 R ) in a 1.4-day orbit around L 168-9 (TOI-134), a bright M1V dwarf (V = 11, K = 7:1) located at 25.15 0.02 pc. The± host star⊕ was observed in the first sector of the Tran- siting Exoplanet Survey Satellite (TESS) mission. For confirmation± and planet mass measurement purposes, this was followed up with ground-based photometry, seeing-limited and high-resolution imaging, and precise radial velocity (PRV) observations using the HARPS and Magellan/PFS spectrographs. By combining the TESS data and PRV observations, we find the mass of L 168-9 b to be +0:44 4.60 0.56 M and thus the bulk density to be 1:74 0:33 times higher than that of the Earth. The orbital eccentricity is smaller than 0.21± (95% confidence).⊕ This planet is a level one candidate− for the TESS mission’s scientific objective of measuring the masses of 50 small planets, and it is one of the most observationally accessible terrestrial planets for future atmospheric characterization. Key words. stars: individual: L 168-9 – planetary systems – stars: late-type – techniques: photometric – techniques: radial velocities 1. Introduction Telescope (ELT, de Zeeuw et al. 2014) will have unprecedented capabilities in performing detailed studies of the atmospheres Transiting planets are the best planet candidates for perform- of terrestrial planets, and the interpretation of the results will ing detailed characterizations, first and foremost, because they require an accurate mass measurement (e.g., Batalha et al. allow for the possibility of unambiguous mass measurements 2019). (e.g., HD 209458b, Charbonneau et al. 2000; Mazeh et al. 2000; Scientific operations in the Transiting Exoplanet Survey Henry et al. 2000). We can determine the minimum mass of Satellite (TESS; Ricker et al. 2015) started in July 2018; the aim the planet (m sin i) from the Doppler effect and also the plane- of which is to detect transiting planets around bright and nearby tary radius and the orbital inclination (i) from the transit light stars that are bright enough for Doppler mass measurements. For curve, thus yielding a measurement of the planet’s mass. More- this task, TESS surveys about 85% of the sky during the prime over, from this combination, we can calculate the planet’s mean mission. The survey covering the southern ecliptic hemisphere is density and shed light on its internal structure by comparing it now complete, and the northern survey is underway. Each hemi- with models containing different amount of iron, silicates, water, sphere is divided into 13 rectangular sectors of 96◦ 24◦ each. hydrogen, and helium. Furthermore, transiting planets are unique Each sector is continuously observed for an interval× of 27-days, because of the feasibility in characterizing the upper atmosphere with a cadence of 2 min for several hundreds of thousands of by spectroscopy during transits and occultations of a signifi- preselected stars deemed best suited for planet searching. Addi- cant number of planets. The forthcoming James Webb Space tionally, during the TESS prime mission, the full frame images, Telescope (JWST, Gardner et al. 2006) and the Extremely Large which consist of the full set of all science and collateral pixels across all CCDs of a given camera, are available with a cadence ? Full Tables B.1 and B.2 are only available at the CDS via anony- of 30 min. M dwarfs are of special interest because the transit mous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http:// and radial-velocity signals of a given type of planet are larger cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/636/A58. for these low-mass stars than they are for Sun-like stars. In addi- ?? Partially based on observations made with the HARPS instrument on the ESO 3.6 m telescope under the program IDs 198.C-0838(A), tion, compared to hotter stars, M dwarfs present better conditions 0101.C-0510(C), and 1102.C-0339(A) at Cerro La Silla (Chile). for the detection of planets orbiting the circumstellar habitable ??? This paper includes data gathered with the 6.5 m Magellan zone: performing surveys in M dwarfs is less time consuming, Telescopes located at Las Campanas Observatory, Chile. and there are larger Doppler signals and an increased transit ???? NASA Hubble Fellow. probability. Sullivan et al.(2015) anticipates that out of the 556 Article published by EDP Sciences A58, page 1 of 13 A&A 636, A58 (2020) small (<2 R ) transiting planets discovered by TESS, 23% of Table 1. L 168-9 (TIC 234994474) properties. ⊕ them will be detected orbiting bright (KS < 9) stars and that 75% of small planets will be found around M dwarfs. Parameter Units Value Reference This paper reports the discovery of a small planet orbiting the star L 168-9 (TOI-134), based on TESS data. The host star RA [J2000] 23h20m07:52s Gaia2018 is a bright M dwarf. An intense precise radial-velocity cam- Dec [J2000] 60◦03054:6400 Gaia2018 paign with HARPS and the Planet Finder Spectrograph (PFS) Spectral type− M1V Ga2014 has revealed the terrestrial nature of the newly detected world. B [mag] 12.45 0.19 Ho2000 This work is presented as follows: Sect.2 describes the host V [mag] 11.02 ±0.06 Ho2000 star properties. Sections 3.1 and 3.3 describe the photometric B [mag] 12.460± 0.025 He2016 A ± and radial-velocity observations. Section4 presents an analy- VA [mag] 11.005 0.018 He2016 sis of all the data, including the study of stellar activity. Finally, g [mag] 11.752 ±0.032 He2016 A ± Sect.6 places L 168-9 b within the larger context of the sample RA [mag] 10.416 0.028 He2016 of detected planets. ± iA [mag] 9.675 He2016 W [mag] 6.928 0.060 Cu2013 1 ± 2. L 168-9 W2 [mag] 6.984 0.020 Cu2013 W [mag] 6.906± 0.016 Cu2013 L 168-9, also known as CD-60 8051, HIP 115211, 2MASS 3 W [mag] 6.897 ± 0.074 Cu2013 J23200751-6003545, with the entry 234994474 of the TESS 4 T 9.2298 ± 0.0073 St2018 input catalog (TIC) or 134 of the TESS object of interest (TOI) ± list, is a red dwarf of spectral type M1V. It appears in the J 7.941 0.019 Cu2003 H 7.320 ± 0.053 Cu2003 southern sky and resides at a distance of 25.150 0.024 pc ± from the Sun (Gaidos et al. 2014; Gaia Collaboration± 2018). Ks 7.082 0.031 Cu2003 B 11.2811± 0.0016 Gaia2018 Table1 lists the key parameters of the star, namely its posi- p ± tion, visual and near-infrared apparent magnitudes, parallax, G 10.2316 0.0008 Gaia2018 R 9.2523 ±0.0011 Gaia2018 proper motion, secular acceleration, and its essential physical p ± properties. π [mas] 39.762 0.038 Gaia2018 Distance [pc] 25.150 ± 0.024 Gaia2018 We performed an analysis of the broadband spectral energy 1 ± distribution (SED) together with the Gaia DR2 parallax in order µα [mas yr− ] 319.96 0.10 Gaia2018 1 − ± to determine an empirical measurement of the stellar radius, fol- µδ [mas yr− ] 127.78 0.12 Gaia2018 dv =dt [m s 1 yr 1] 0.06865− ±0.00011 this work lowing the procedures described by Stassun & Torres(2016) r − − ± and Stassun et al.(2017, 2018a). We took the B V magnitudes Ms [M ] 0.62 0.03 Ma2019 T T ± from Tycho-2, the BVgri magnitudes from APASS, the JHKS Rs [R ] 0.600 0.022 Sect.2 T [K] 3800± 70 Sect.2 magnitudes from 2MASS, the W1–W4 magnitudes from WISE, eff ± and the G magnitude from Gaia. Together, the available pho- Ls [L ] 0.0673 0.0024 Sect.2 3 ± tometry spans the full stellar SED over the wavelength range of log(g) [g cm− ] 4.04 0.49 Sect.2 ± 0.35–22 µm (see Fig.1). [Fe=H] 0.04 0.17 Ne2014 ± We performed a fit using NextGen stellar atmosphere mod- log(R0 ) 4.562 0.043 As2017A HK − ± els (Hauschildt et al. 1999); the effective temperature (T ) and Prot [days] 29:8 1:3 Sect.
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